Propagating slow magneto-acoustic waves are commonly observed in different coronal structures but are most prominent in active region fan loops. Their rapid damping with damping lengths of the order of a wavelength has been investigated in the past by several authors. Although different physical mechanisms have been proposed, significant discrepancies between the theory and observations remain. Recent high-resolution observations captured simultaneously by two different instruments reveal distinct damping lengths for slow magneto-acoustic waves although their passbands are similar. These results suggest a possible contribution of instrumental characteristics on the measurement of damping lengths. Here, we analyse the behavior of slow waves using a different pair of instruments in order to check the prevalence of such results. In particular, the cotemporal observations of active region NOAA AR12712 by the High-Resolution Coronal Imager (Hi-C 2.1) and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) are utilised. The estimated oscillation periods of slow magneto-acoustic waves identified from these data are 2.7{ \,}$\pm${ \,}0.2{ \,}min from SDO/AIA, and 2.8{ \,}$\pm${ \,}1.2{ \,}min from Hi-C 2.1. The corresponding propagation speeds are found to be 46.0{ \,}$\pm${ \,}1.7{ \,}km{ \,}s$^{ -1}$ and 48.1{ \,}$\pm${ \,}0.6{ \,}km{ \,}s$^{ -1}$, respectively. Damping lengths were calculated by two different methods, the Phase Tracking Method (PTM) and the Amplitude Tracking Method (ATM). The obtained values from PTM are 4.0{ \,}$\pm${ \,}2.1{ \,}Mm and 4.1{ \,}$\pm${ \,}0.3{ \,}Mm while those from ATM are 3.4{ \,}$\pm${ \,}1.0{ \,}Mm and 3.7{ \,}$\pm${ \,}0.1{ \,}Mm, respectively, for the AIA and Hi-C data. Our results do not indicate any notable difference in damping lengths between these instruments.
Categories: astro-ph.SR